Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.4804c&link_type=abstract
American Astronomical Society, 186th AAS Meeting, #48.04; Bulletin of the American Astronomical Society, Vol. 27, p.879
Astronomy and Astrophysics
Astronomy
Scientific paper
We studied the gamma-ray emission mechanisms from pulsars with period, P, between 4.6 times 10(-2) B12(2/5) s and 0.17 B12(5/12) sin (1/6) theta alpha (-5/4) s in terms of outermagnetospheric gap model. We found that the spectra of all known gamma -ray pulsars can be fitted by two free parameters, namely, alpha r_L, the mean distance to the outergap, and sin theta , the mean pitch angle of the secondary e(+/-) pairs. Gamma-rays from those pulsars with P < 0.17 B12(5/12) sin (1/6) alpha (-5/4) s are mainly emitted by secondary e(+/-) pairs, which are created beyond the outergap, via synchrotron radiation and the gamma-ray emission efficiency is ~ 10(-2) . For pulsars with period approaching ~ 0.17 B12(5/12) sin (1/6) alpha (-5/4) s, their gamma-ray emission efficiency is approaching unity. We used our model to fit the observed spectra of gamma -ray pulsars (Vela, PSR1706-44, PSR1055-52, PSR1509-58, Geminga). All the best fit curves satisfy the constraints of alpha and sin theta . The pulse separation and relative intensity of pulses are function of alpha . In our model, the first three strongest theoretical gamma -ray sources have been detected. PSR1951+32 is predicted to be the fourth strongest gamma -ray pulsar (Cheng and Ding, 1994, ApJ, 432, 724) which is confirmed by the recent GRO result.
Cheng Kwong Sang
Ding Winnis K. Y.
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